Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

亚,超声速旋涡流动特征的定性分析研究

本文研究了沿其轴向运动的亚声速和超声速旋涡的性状，指出两者完全不同。在加速区，于涡轴附近，亚声速旋涡的横截面流线即横截面上的速度场的向量线为由外向内转的稳定螺旋点形态，空间流线沿其轴向是收缩的，而超声速旋涡的横截面流线为由内向外转的不稳定螺旋点形态，空间流线沿其轴向是散开的。在减速区，两者的情况也恰好相反，此外，当旋涡由加速区过渡到减速区时，两者横截面流线方程在涡轴附近的Ｈｏｐｆ分叉情况也不同，亚     

固冲发动机补燃室流场的实验校测

1引言目前数值模拟已广泛应用到火箭发动机的流场分析中,特别是固冲发动机补燃室的燃烧和流动[1,2]。但是这种方法在固冲发动机补燃室应用的有效性还没有合适的实验验证。国外开展的补燃室流动实验大多以水为介质,用片光流动显示的方法观察流场的概貌,与真实发动机的流动之间存     

计算跨声速机翼尾涡流自适应区域方法

本文利用自适应区域方法调节机翼后每个Ｔｒｅｆｆｔｚ平面上的计算域，使得尾涡对这个计算域边界的影响足够小，从而提高了计算的精度和时间。考虑到间断面的影响，在尾涡面上引入有旋项对流场进行计算。椭圆载荷机翼计算表明本文计算结果与经典Ｂｅｔｚ理论一致。用本文方法对某轰炸机进行了计算，计算结果已用于预计其实际飞行的尾涡面。     

风洞中复杂流场三维速度LDV测量

本文将一台TSI 9100-7型两分量激光测速仪改进为可测三个速度分量的LDV系统,并用于测量风洞中椭球体模型、双三角翼模型大迎角下的复杂流场三维速度分量。流场横截面内的速度矢量分布与相同实验条件下的流态显示结果相符合,并对涡流场加以分析。     

漩涡发生器对燃油喷嘴的雾化性能影响的数值研究

为了探讨漩涡发生器(简称V.G)对燃油喷嘴雾化性能的影响,利用Gambit分别建立了原型喷嘴、加装2个漩涡发生器和加装4个漩涡发生器喷嘴的模型,并利用FLUENT软件进行了数值模拟,得到了三种模型的出口流场分布图。计算结果表明:在相同燃油压力下,加装漩涡发生器可以加快射流的混合速度,其中加装4个漩涡发生器的喷嘴的加速掺混能力最高,加装2个的其次,但仍比"原型"的情况有明显的改善;当燃油压力改变时,掺混能力会随着燃油压力的提高而提高。     

环形燃烧室性能计算

在任意曲线坐标系下对包括扩压器和火焰筒在内的环形燃烧室三维两相反应流进行了数值模拟。燃烧室性能采用多维经验分析法估算所用的数学模型有 κ-ε,紊流模型 ,EBU -Arrhenius紊流燃烧室模型 ,六通量热辐射模型以及颗粒群轨道模型。在非交错网格体系下 ,气相采用 SIMPLE算法和液相采用 PSIC算法求解 ,通过两种工况和三种扩压器进口速度分布计算表明 ,所得的流场各气流参数分布和燃烧室性能较合理 ,本文所建立的程序可为燃烧室优化设计和研制提供有用数据。     

大迎角三角翼旋涡运动及其破碎特性的数值研究

从流体力学的基本方程出发，利用Ｈａｌｌ的涡核准柱假设，导出反映涡核运动的Ｎ－Ｓ方程。采用差分方法计算旋涡流场，进而分析三角翼上前缘分离涡的运动特点及其破碎机下。从计算结果可以看出，旋涡的轴向速度向下游逐渐下降，且涡心处于降较快，外缘下降较慢，反映了粘性作用自涡心外缘逐渐下降的特点；涡核外缘的径向速度开始为负，说明开始阶段有流体流入涡核，随着旋涡向下游运动，径向速度有所增加，到一定位置后增加迅速，说     

双圆柱斜向排列时旋涡脱落频率的实验研究

本研究用热线风速仪测量了斜向排列双圆柱的尾迹,并分析了尾迹中某些特征点上的速度频谱,从旋涡脱落频率的规律来研究双圆柱绕流相互之间的干扰。当两圆柱间距较远时,速度振荡的频率与单圆柱卡门涡街的频率相接近,随着两圆柱间距的接近,前、后圆柱各有其不同的旋涡脱落频率,且都不同于单圆柱旋涡脱落的频率。特别是当两圆柱处于某一相对位置时,出现双峰值的功率谱,其中一个峰值的频率大大地高于另一个峰值对应的频率,而且这两个峰值谁主谁副是不确定的,呈现出不稳定流动的特性。     

空中受油管的绕流特性研究

空中加油是提高飞机航程、活动半径的重要方法。通过对四种固定受油管的数值模拟,从流动特性的改进方面说明了合适的截面及倾角会降低受油管绕流的压力脉动,进而使噪声降低。